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REVIEW 2 major objections 8 minor 300 references

Sub-Saturns in the Neptunian desert and ridge lack nearby companions like hot Jupiters, while savanna ones sit in compact multi-planet systems like warm Jupiters, pointing to two migration channels.

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2026-07-13 02:54 UTC pith:JDHTOX2D

load-bearing objection Solid first dual-method companion census of sub-Saturns; the desert/ridge vs savanna contrast is large, well-tested, and carries the claim even when absolute rates move with the prior. the 2 major comments →

arxiv 2607.09451 v1 pith:JDHTOX2D submitted 2026-07-10 astro-ph.EP

Companion Architectures of Sub-Saturns: Distinct Migration Pathways Across the Neptunian Landscape

Luis Thomas , Louise D. Nielsen , Alex J. Cridland , Martin Schlecker , Sydney Vach This is my paper
classification astro-ph.EP
keywords sub-SaturnsNeptunian desertNeptunian ridgeplanet migrationcompanion occurrencehigh-eccentricity migrationradial velocitytransit photometry
verification ladder T0 review T1 audit T2 compute T3 formal T4 reserved

The pith

A machine-rendered reading of the paper's core claim, the machinery that carries it, and where it could break.

Close-in sub-Saturns are not evenly spread: they are scarce in the Neptunian desert, piled up in a narrow ridge at periods of about 3–6 days, and more moderately common farther out in the savanna. This paper asks whether those landscape regions also differ in the planets that share their systems. After building per-system maps of what companions the available transit and radial-velocity data could have found, and correcting the raw counts with a Poisson-Binomial model, the authors find a sharp split. About 70% of savanna sub-Saturns have nearby companions (periods under 200 days), versus only about 10% of desert and ridge sub-Saturns; rates of systems with more than one companion follow the same pattern. The nearby companions that do exist are almost all small, so the sub-Saturn is usually the dominant body of its inner system. Desert and ridge systems therefore look dynamically emptied in the same way hot Jupiters do, while savanna systems look like the compact multis of warm Jupiters. The authors read this as evidence that high-eccentricity migration delivered the desert and ridge planets and that quiescent disk migration or in-situ formation populated the savanna, two channels operating inside one population.

Core claim

After completeness correction, savanna sub-Saturns show high rates of nearby companions (69.9+6.9/−7.7%) and of multiple companions (64.4+8.9/−9.8%), while desert and ridge sub-Saturns show low rates (10.5+7.8/−5.3% and 14.9+13.7/−9.1%). Those contrasts match the known companion architectures of warm and hot Jupiters and remain when the sample is cut by radius, density, eccentricity, and host-star properties. The paper therefore claims two migration pathways within the sub-Saturn population: high-eccentricity migration into the desert and ridge, and quiescent assembly into the savanna.

What carries the argument

Combined RV-plus-transit detection probability surfaces, averaged into a regional completeness Cj under a log-uniform companion distribution, and fed into a Poisson-Binomial likelihood that converts binary detections and non-detections into occurrence fractions f = 1 − e−μ (or the ≥2 analogue).

Load-bearing premise

The correction for missing companions assumes those companions are spread evenly in log period and log mass inside each search box; changing that assumed shape moves the absolute rates a lot even though the desert-ridge versus savanna contrast stays.

What would settle it

A larger sample of desert and ridge sub-Saturns with deep enough RV and transit sensitivity that the nearby-companion rate either rises to match the savanna rate or stays near the hot-Jupiter floor of roughly 10 percent, independent of the assumed mass–period distribution of undetected planets.

Watch this falsifier — get emailed when new claim-graph text bears on it.

If this is right

  • Desert and ridge sub-Saturns should be treated as dynamically hot systems whose present-day orbits were set by high-eccentricity migration, not as quiet disk-migration survivors.
  • Savanna sub-Saturns should be expected to keep compact multi-planet architectures, so future surveys can use multiplicity as a landscape diagnostic.
  • The parallel with hot and warm Jupiters implies that intermediate-mass and giant planets share the same two delivery channels rather than forming a separate evolutionary sequence of stripped hot Jupiters.
  • Bulk density and residual eccentricity can further tag migration channel inside the savanna, with dense or eccentric savanna planets more likely to sit in emptied systems.

Where Pith is reading between the lines

These are editorial extensions of the paper, not claims the author makes directly.

  • If the same completeness pipeline is run on a pure hot-Jupiter sample with identical period and mass cuts, the nearby-companion rate should land near the 10% desert–ridge number; a large mismatch would weaken the shared-migration reading.
  • Stellar companions capable of Kozai cycles are not counted in the massive-planet category here; folding them in could raise the inferred HEM-perturber fraction without changing the nearby-planet deficit.
  • The claim that absolute rates depend on the assumed companion distribution suggests a useful follow-up: re-infer the rates jointly with a free power-law slope on mass and period and report the marginal landscape contrast.

Editorial analysis

A structured set of objections, weighed in public.

Desk editor's note, referee report, simulated authors' rebuttal, and a circularity audit.

Referee Report

2 major / 8 minor

Summary. The paper measures completeness-corrected companion occurrence rates for 90 well-characterized sub-Saturns (4–8.5 R⊕) in 86 systems spanning the Neptunian desert, ridge, and savanna. Using joint RV (RVSearch injection–recovery) and transit (BLS on TESS/Kepler/K2) completeness maps, Monte-Carlo combination with an empirical mutual-inclination prior, and a Poisson-Binomial likelihood, the authors find a large architectural contrast: after correction, ~70% of savanna sub-Saturns have nearby (P<200 d) companions versus ~10% of desert+ridge systems, with multiple-companion rates ~64% versus ~15%. Nearby companions that exist are almost exclusively small (M<20 M⊕). Crosscuts in radius, density, eccentricity, and host properties leave the landscape gradient intact. The authors interpret desert/ridge systems as dynamically emptied (HEM-like, matching hot Jupiters) and savanna systems as compact multi-planet (disk migration/in situ, matching warm Jupiters).

Significance. If the contrast holds, this is a strong dynamical tracer that sub-Saturns are not a single migration channel: desert and ridge track high-eccentricity delivery while the savanna tracks quiescent assembly. The parallel to hot versus warm Jupiter companion rates is a concrete, falsifiable link between intermediate-mass and giant-planet migration. Methodological strengths include per-system dual-method completeness, a Poisson-Binomial treatment that correctly handles multi-companion systems, independent validation with Beta-Binomial, Poisson-process, and ABC-PMC frameworks (App. A.1), prior and intrinsic-distribution stress tests (App. A.2–A.3), and an explicit RV follow-up selection-function analysis (§5.3). These make the relative landscape contrast unusually well stress-tested for an occurrence-rate study of this sample size.

major comments (2)
  1. Abstract and §4.1 quote absolute nearby and multiple rates (e.g. 69.9% vs 10.5%) as headline results, but §3.4 Eq. (5) and App. A.3 show that integrated completeness Cj assumes companions uniform in (log P, log M) within each category region. Under Cumming et al. (2008) or rising-small alternatives, absolute rates of broad, low-completeness categories shift by tens of percentage points (Table A.3: nearby desert+ridge 10.5%→20.4%→36.7%; savanna 69.9%→89.2%→98.1%). The desert+ridge versus savanna contrast is preserved, which carries the scientific claim, but the abstract and main-text numerical claims should state explicitly that absolute fractions are conditional on the log-uniform baseline and that only the relative contrast is robust under the tested alternatives.
  2. §4.1 combines desert (N=9) and ridge (N=28.5) after stating that their posteriors “agree within 1σ across companion classes.” With desert N=9 and mean completeness ~34–53%, the desert-only posteriors are extremely broad (e.g. nearby 11.3+16.0/−8.4%; any companion 34.0+21.8/−17.9%; Table 1), so 1σ agreement is weakly informative. The combination is motivated by prior density and metallicity work and is reasonable for the main contrast, but the manuscript should not overstate independent statistical agreement between desert and ridge; a short statement that desert alone is too sparse to test equality, and that the combined bin is adopted on external grounds, would be more accurate.
minor comments (8)
  1. Fig. 2 caption says “as a function of orbital period” but the panels are 2D (P, mass/radius) completeness maps; clarify axes and color scale in the caption.
  2. §3.1: the FAP threshold of 1% and the recovery criterion for known planets that are not recovered blindly (parameters passed in by hand) should be stated more explicitly as a potential incompleteness floor for very low-K known planets.
  3. §3.3 Eq. (1): imposing a hard floor of 8 R⊕ for Mp≥127 M⊕ is reasonable; note briefly whether results for giant nearby companions are sensitive to that floor.
  4. §5.2: the comparison of massive long-period rates to hot-Jupiter literature (~50–70%) is carefully caveated as a lower limit (P<10^4 d, resolved orbits only). Consider moving one sentence of that caveat into the abstract or conclusions so the “match hot Jupiters” phrasing is not over-read for outer companions.
  5. Table 1 and subsequent tables: non-integer weighted counts (e.g. 1.5/37.5) are correct under the 1/nss weighting but may confuse readers; a footnote restating the weighting once is enough.
  6. Throughout: “Pl_N > 2” in figure legends for multiple companions is unclear notation; prefer “N_pl ≥ 3” or “≥2 companions.”
  7. Sample size in abstract says 86 systems; §2 says 90 sub-Saturns in 86 systems — consistent, but the abstract could say “90 sub-Saturns in 86 systems” to match the body.
  8. A few reference formatting inconsistencies (e.g. Stefànsson vs Stefánsson; mixed arXiv-only citations for 2025–2026 papers) should be cleaned for production.

Circularity Check

0 steps flagged

No significant circularity: occurrence rates are measured from detections against independent completeness maps; the HEM/quiescent interpretation is an external theoretical mapping, not forced by construction.

full rationale

The paper's load-bearing result is an empirical contrast in completeness-corrected companion fractions (nearby P<200 d: 69.9% savanna vs 10.5% desert+ridge; multiple: 64.4% vs 14.9%) obtained by injection-recovery completeness maps plus a Poisson-Binomial likelihood on binary detection outcomes (Sect. 3.3–3.4, Eqs. 4–10, Table 1, Fig. 3). Landscape bins are taken from Castro-González et al. (2024a) as an external period cut, not defined from the companion data. Absolute rates inherit the log-uniform companion prior inside each category region (Eq. 5), but App. A.3 shows both populations share the same maps and assumption, so the relative contrast survives alternative distributions, priors, and three independent statistical frameworks (Tables A.1–A.3). Crosscuts by radius, density, eccentricity, and host properties leave the landscape gradient intact; RV follow-up selection is shown not to drive multiplicity (Sect. 5.3). The mapping of low nearby-companion rates onto HEM (and high rates onto disk migration) is an external theoretical expectation drawn from the broader literature (Rasio & Ford 1996; Mustill et al. 2015; Dawson & Johnson 2018; hot/warm Jupiter companion statistics), not a mathematical identity inside the paper. Self-citations (Thomas et al. 2025a,b) appear only in secondary crosscuts and do not force the central contrast. No step reduces a claimed prediction to a fitted input or to a self-citation uniqueness claim by construction.

Axiom & Free-Parameter Ledger

8 free parameters · 6 axioms · 0 invented entities

The central demographic contrast rests on standard exoplanet detection statistics plus a handful of literature calibrations (landscape boundaries, mass-radius relation, mutual inclinations) and analysis choices (period/mass category cuts, log-uniform companion prior). No new physical entities are postulated; the migration interpretation is an external mapping of the measured rates onto existing HEM and disk-migration theory.

free parameters (8)
  • Nearby-companion period cut = 200 d
    Pcomp < 200 d is an analysis choice that defines the main diagnostic category; results are reported only for this cut.
  • Massive long-period cuts = 1 MJup, 365 d
    Mc ≥ 1 MJup and Pc > 365 d define the outer-perturber category used to test HEM drivers.
  • Companion mass bins = 20 M⊕, 80 M⊕
    Small/medium/giant boundaries at 20 and 80 M⊕ control the claim that the landscape gradient is driven by small planets.
  • Density split = 1.4 g cm−3
    ρ = 1.4 g cm−3 taken from the literature bimodality minimum and used for the density crosscut.
  • Radius split = 6 R⊕
    Rp = 6 R⊕ from the envelope-mass-fraction gap of Thomas et al. 2025b, used for the Neptune-like versus giant-like crosscut.
  • Eccentricity split = 0.1
    e = 0.1 boundary used to separate circular versus eccentric sub-samples.
  • Host metallicity and mass splits = [Fe/H]=0.17, 1.0 M⊙
    Median [Fe/H] = 0.17 and M⋆ = 1.0 M⊙ used for stellar-property crosscuts.
  • Injection-recovery thresholds = FAP=1%, S/Npink=8, ΔP=5%
    FAP 1% for RVSearch, S/Npink ≥ 8 and 5% period match (plus harmonics) for BLS recovery are fixed analysis choices that set the completeness surfaces.
axioms (6)
  • domain assumption Neptunian desert/ridge/savanna period boundaries (P=3.2 d, 5.7 d) correctly partition distinct populations
    Adopted from Castro-González et al. 2024a and used to define all landscape bins (Sect. 2).
  • domain assumption Müller et al. 2024 mass-radius relation (with 8 R⊕ floor for giants) converts between RV (P,K) and transit (P,Rp) completeness maps
    Eq. 1 and surrounding text in Sect. 3.3; required to build combined completeness surfaces.
  • domain assumption Empirical mutual-inclination distribution of He et al. 2020 (Rayleigh scale set by multiplicity) describes the relative orientation of companions
    Sect. 3.3 Eqs. 2–3; controls geometric transit probability in the Monte-Carlo combination.
  • domain assumption True number of companions per system in a category is Poisson(μ) with common μ inside each landscape bin
    Poisson-Binomial model of Sect. 3.4; validated but not proven by the three alternative methods in App. A.1.
  • ad hoc to paper Undetected companions are distributed uniformly in (log P, log M) inside each category region when computing integrated completeness Cj
    Explicit baseline of Sect. 3.4 and App. A.3; absolute rates are sensitive to this choice.
  • domain assumption A short present-day orbital period alone does not generically suppress nearby companions (ultra-short-period and Kepler multi statistics)
    Sect. 5.1 argument that the companion deficit is mass-dependent rather than period-generic.

pith-pipeline@v1.1.0-grok45 · 55179 in / 3984 out tokens · 59824 ms · 2026-07-13T02:54:47.496864+00:00 · methodology

0 comments
read the original abstract

Close-in sub-Saturns (4 - 8.5 R$_\oplus$) are depleted in the Neptunian desert, accumulate in a narrow overdensity near P = 3.2 - 5.7 d (the Neptunian ridge), and thin out into the more moderately populated savanna at longer periods. We test whether sub-Saturns have systematically different companion architectures, as predicted if desert and ridge planets arrived through high-eccentricity migration while savanna planets migrated quiescently. We compile 86 systems with both transit and RV data, construct completeness maps and combine them into detection probability surfaces for companions. The combined completeness maps are used to calculate companion occurrence rates across different companion types with a Poisson-Binomial framework. Companion architectures differ significantly across the landscape. $69.9_{-7.7}^{+6.9}\%$ of savanna sub-Saturns have nearby companions (P < 200 d) compared to only $10.5_{-5.3}^{+7.8}\%$ of desert and ridge sub-Saturns. Additionally, sub-Saturns in the savanna often reside in multi-planet systems with $64.4_{-9.8}^{+8.9}\%$ having more than one companion planet versus only $14.9_{-9.1}^{+13.7}\%$ in the desert and ridge. In both populations, the nearby companions that do exist are almost exclusively small (M < 20 M$_\oplus$), meaning the sub-Saturn is typically the dominant body of its inner system. These contrasts are robust to crosscuts in sub-Saturn radius, bulk density, eccentricity, and host-star properties. Desert and ridge sub-Saturns reside in dynamically emptied systems whose nearby companion rates match those of hot Jupiters, while savanna sub-Saturns inhabit compact multi-planet systems resembling those of warm Jupiters. This parallel supports two migration channels operating within a single population: HEM delivering planets to the desert and ridge, and quiescent disk migration or in-situ formation populating the savanna.

Figures

Figures reproduced from arXiv: 2607.09451 by Alex J. Cridland, Louise D. Nielsen, Luis Thomas, Martin Schlecker, Sydney Vach.

Figure 1
Figure 1. Figure 1: Orbital architecture plots of the 86 systems in our sample ordered by the position of the closest sub-Saturn in the Neptunian landscape. Filled circles are sub-Saturns colored by their position within the Neptunian landscape. Unfilled circles indicate com￾panion planets with the size of the circle indicating the mass of the companion. then perform an injection–recovery analysis, injecting 10,000 synthetic … view at source ↗
Figure 2
Figure 2. Figure 2: Completeness maps of our injection–recovery analysis for the RV data (top row), the photometric data (middle row) and the combination of both datasets (bottom row). Plotted are the average completeness values as a function of orbital period for the sub￾Saturn systems in the sample divided into the desert (left column), ridge (middle column) and savanna (right column) subsamples. Because the occurrence frac… view at source ↗
Figure 3
Figure 3. Figure 3: Posterior distributions of the completeness-corrected occurrence rates of different types of companions for systems with a known sub-Saturn in the desert or ridge (purple) or savanna (green). panion rate is 76.4 +7.0 −8.1% in the savanna versus 8.8 +9.4 −5.6% in the desert+ridge, following a similarly strong trend as the multiple companion rate. For high-density sub-Saturns, on the other hand, the landscap… view at source ↗
Figure 4
Figure 4. Figure 4: Posterior distributions of the completeness-corrected occurrence rates of different types of companions for systems with a Neptune-like (4 R⊕ ≤ Rp < 6 R⊕) or giant-like (6 R⊕ ≤ Rp ≤ 8.5 R⊕) sub-Saturn. The different sub-Saturn classes are further divided by their location within the Neptunian landscape. dynamically hot (e > 0.1) orbits (Dong et al. 2021; Morgan et al. 2026; Schlecker et al. 2020; Eberhardt… view at source ↗
Figure 5
Figure 5. Figure 5: Posterior distributions of the completeness-corrected occurrence rates of different types of companions for the two density classes: low-density (ρ < 1.4 g cm−3 ) and high-density (ρ ≥ 1.4 g cm−3 ). The different density classes are further divided by their location within the Neptunian landscape. companion rate is 54.1 +8.9 −9.1% for metal-poor hosts compared to 43.0 +9.4 −9.1% for metal-rich hosts, and t… view at source ↗
Figure 6
Figure 6. Figure 6: Posterior distributions of the completeness-corrected occurrence rates of different types of companions for the two eccentric￾ity classes: circular (e < 0.1) and eccentric (e ≥ 0.1). The different eccentricity classes are further divided by their location within the Neptunian landscape. and inner categories at q ≤ 0.003, the any category at q = 0.014, and the outer category marginally at q = 0.050; all six… view at source ↗
Figure 7
Figure 7. Figure 7: Distribution of host star masses for sub-Saturns in the desert and ridge (purple) compared to the savanna (green). Sa￾vanna sub-Saturn hosts cluster around ∼ 1 M⊙ while desert and ridge hosts extend to M dwarfs. in the desert and ridge has a different companion architecture. They lack nearby companions (10.5 +7.8 −5.3%) and rarely have more than one companion (14.9 +13.7 −9.1 %). This pattern is the expect… view at source ↗
Figure 8
Figure 8. Figure 8: Association between system properties and the presence of detected companions from the model-free two-sample tests. Panel (a): Anderson-Darling; panel (b): Kolmogorov-Smirnov (permutation p-values on the raw detection labels). Bold entries mark p < 0.05; a ‘+’ marks associations that remain significant after false-discovery-rate control at q < 0.05. nor surviving population of low-density sub-Saturns even … view at source ↗

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